Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.45cm,clip]{7936fig1.ps}\end{figure}$ Figure 1: Measured He I 10 830 Å emission profiles for increasing distances to the solar limb, scanning a broad range of the height extension of the spicules. Each profile is the average of the 312 pixels along the slit (which was always kept parallel to the limb).
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{7936fig2.ps}\end{figure}$ Figure 2: 3D representation of the measured He I 10 830 Å emission profiles for increasing distances to the solar visible limb. Note that the x-axis is wavelength, the y-axis the height above solar limb and the z-axis the intensity normalised to the maximum emission in the line centre of the red component.
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In the text

$\begin{figure} \par\includegraphics[width=8.45cm,clip]{7936fig3.ps}\end{figure}$ Figure 3: Determination of the blue and red components of the He I 10 830 Å triplet from the observed emission profiles. In this example the slit was placed at 1 $.\!\!^{\prime\prime}$ 4 off the solar visible limb. See text for details. The solid line represents the average emision profile. The dotted line is the Gaussian fit to the symmetrised red component. Subtraction of this from the observed profile leaves the blue component, which is also fitted by a Gaussian profile (thin solid line). The sum of both Gaussians (dashed line) gives the fit to the observed profile.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7936fig4.ps}\end{figure}$ Figure 4: Measured ratio $\cal R$ = $I_{\rm blue}/I_{\rm red}$ as a function of distance to the solar limb. Thin lines come from each pixel along the slit. The thick solid line represents the average and the dashed line the value of the optically thin regime.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7936fig5.ps}\end{figure}$ Figure 5: Observed (average) vs. theoretical variation of the ratio $\cal R$ = $I_{\rm blue}/I_{\rm red}$ with height.
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In the text

$\begin{figure} \par\includegraphics[width=8.45cm,clip]{7936fig1.ps}\end{figure}$	Figure 1: Measured He I 10 830 Å emission profiles for increasing distances to the solar limb, scanning a broad range of the height extension of the spicules. Each profile is the average of the 312 pixels along the slit (which was always kept parallel to the limb).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{7936fig2.ps}\end{figure}$	Figure 2: 3D representation of the measured He I 10 830 Å emission profiles for increasing distances to the solar visible limb. Note that the x-axis is wavelength, the y-axis the height above solar limb and the z-axis the intensity normalised to the maximum emission in the line centre of the red component.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7936fig4.ps}\end{figure}$	Figure 4: Measured ratio $\cal R$ = $I_{\rm blue}/I_{\rm red}$ as a function of distance to the solar limb. Thin lines come from each pixel along the slit. The thick solid line represents the average and the dashed line the value of the optically thin regime.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7936fig5.ps}\end{figure}$	Figure 5: Observed (average) vs. theoretical variation of the ratio $\cal R$ = $I_{\rm blue}/I_{\rm red}$ with height.
Open with DEXTER